Abundance analysis of targets for the COROT/MONS asteroseismology missions

Bruntt, H.; Catala, C.; Garrido, R.; Rodríguez‐López, C.; Stütz, Ch.; Knoglinger, P.; Mittermayer, P.; Bouret, Jean-Claude; Hua, T.; Lignières, F.; Charpinet, S.; Veer-Menneret, C. van 't; Ballereau, D.

doi:10.1051/0004-6361:20020549

Cited by 51 publications

(68 citation statements)

References 20 publications

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“…We found v sin i = 70 km s −1 using Hα and v sin i = 80 km s −1 using H β . This is in good agreement with the value of v sin i = 84 km s −1 measured by Bruntt et al (2002).…”

Section: Rotation Of Other Starssupporting

confidence: 91%

Rotation of stars in NGC 6134

Rasmussen¹,

Bruntt²,

Frandsen³

et al. 2002

A&A

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Abstract. We present results of spectroscopic observations of selected stars in the southern open cluster NGC 6134. We have determined the rotational velocities of the six known δ Scuti stars in NGC 6134 as well as several other non-variable stars with similar colour temperature in order to investigate if v sin i and variability is somehow connected: we find no such correlation. We also compare the distribution of v sin i of δ Scuti stars and non-variable stars with four other well-studied open clusters to look for any systematic behaviour, but we find no conclusive evidence for v sin i and variability to be connected. We have also used the spectra to carry out an abundance analysis of the δ Scuti stars in NGC 6134 to confirm the high metal content of the cluster. We find [Fe/H] = +0.38 ± 0.05 which is in agreement with the result obtained from Strömgren photometry. We also present ∆a photometry of the cluster, but we find no chemical peculiar stars based on this index.

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“…We found v sin i = 70 km s −1 using Hα and v sin i = 80 km s −1 using H β . This is in good agreement with the value of v sin i = 84 km s −1 measured by Bruntt et al (2002).…”

Section: Rotation Of Other Starssupporting

confidence: 91%

Rotation of stars in NGC 6134

Rasmussen¹,

Bruntt²,

Frandsen³

et al. 2002

A&A

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“…The method is the same as employed by Dall et al (2005), adopted from the procedures of Morel et al (2003) and Bruntt et al (2002Bruntt et al ( , 2004. The first step is the measurement of the EWs, which is accomplished using DAOSPEC 1 (Stetson & Pancino 2005, in preparation), which uses an iterative Gaussian fitting and subtraction procedure to fit the lines and the effective continuum.…”

Section: Abundance Analysis: Methodsmentioning

confidence: 99%

“…The software is called VWA which has a graphical user interface (GUI). The method and the VWA software have been described in detail by Bruntt et al (2002Bruntt et al ( , 2004 and the method compared to the classical EW method by Bikmaev et al (2002). The abundance analysis relies on atomic parameters from the VALD database (Kupka et al 1999;Piskunov et al 1995) and uses modified ATLAS9 atmospheric models from interpolation in the grid published by Heiter et al (2002).…”

Section: Abundance Analysis: Methodsmentioning

confidence: 99%

Binarity, activity and metallicity among late-type stars

Dall¹,

Bruntt²,

Strassméier

2005

A&A

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We present the first in a series of papers that attempt to investigate the relation between binarity, magnetic activity, and chemical surface abundances of cool stars. In the current paper, we lay out and test two abundance analysis methods and apply them to two well-known, active, single stars, HD 27536 (G8IV-III) and HD 216803 (K5V), presenting photospheric fundamental parameters and abundances of Li, Al, Ca, Si, Sc, Ti, V, Cr, Fe, Co and Ni. The abundances from the two methods agree within the errors for all elements except calcium in HD 216803, which means that either method yields the same fundamental model parameters and the same abundances. Activity is described by the radiative loss in the Ca ii H and K lines with respect to the bolometric luminosity, through the activity index R HK . Binarity is established by very precise radial velocity (RV) measurements using HARPS spectra. The spectral line bisectors are examined for correlations between RV and bisector shape to distinguish between the effects of stellar activity and unseen companions. We show that HD 27536 exhibit RV variations mimicking the effect of a low-mass (m ∼ 4 M J ) companion in a relatively close (a ∼ 1 AU) orbit. The variation is strongly correlated with the activity, and consistent with the known photometric period P = 306.9 d, demonstrating a remarkable coherence between R HK and the bisector shape, i.e. between the photosphere and the chromosphere. We discuss the complications involved in distinguishing between companion and activity induced RV variations.

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“…Strömgren photometry, taken in 2001, confirmed the variability with excess power in the 1 d −1 to 5 d −1 region, but yielded no identifiable frequencies (Bruntt et al 2002). Further spectroscopy by Mathias et al (2004) showed, again, low-amplitude variations in the blue wing of the line profile.…”

Section: Introductionmentioning

confidence: 89%

“…The spectroscopic parameters from these works and those from two further photometric studies by Lastennet et al (2001) and Poretti et al (2005) are given in Table 1. The radius of the star is estimated from 2mass infra-red photometry to be 1.601 ± 0.052 R⊙ (Masana et al 2006) and an estimate of the stellar mass of 1.55 ± 0.14 M⊙ is given in Bruntt et al (2002).…”

Section: Introductionmentioning

confidence: 99%

The classification of frequencies in the γ Doradus/δ Scuti hybrid star HD 49434★

Brunsden

Pollard

Cottrell

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Hybrid stars of the γ Doradus and δ Scuti pulsation types have great potential for asteroseismic analysis to explore their interior structure. To achieve this, mode identifications of pulsational frequencies observed in the stars must be made, a task which is far from simple. In this work we begin the analysis by scrutinizing the frequencies found in the CoRoT photometric satellite measurements and ground-based high-resolution spectroscopy of the hybrid star HD 49434. The results show almost no consistency between the frequencies found using the two techniques and no characteristic period spacings or couplings were identified in either dataset. The spectroscopic data additionally show no evidence for any long term (5 year) variation in the dominant frequency. The 31 spectroscopic frequencies identified have standard deviation profiles suggesting multiple modes sharing (l, m) in the δ Scuti frequency region and several skewed modes sharing the same (l, m) in the γ Doradus frequency region. In addition, there is a clear frequency in the γ Doradus frequency region that appears to be unrelated to the others. We conclude HD 49434 remains a δ Scuti/ γ Doradus candidate hybrid star but more sophisticated models dealing with rotation are sought to obtain a clear picture of the pulsational behaviour of this star.

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Abundance analysis of targets for the COROT/MONS asteroseismology missions

Cited by 51 publications

References 20 publications

Rotation of stars in NGC 6134

Rotation of stars in NGC 6134

Binarity, activity and metallicity among late-type stars

The classification of frequencies in the γ Doradus/δ Scuti hybrid star HD 49434★

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